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Messier 81'S Planck View Vs Its Halo Mapping

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Messier 81'S Planck View Vs Its Halo Mapping Astronomy & Astrophysics manuscript no. M81 c ESO 2018 November 17, 2018 Messier 81’s Planck view vs its halo mapping V.G. Gurzadyan1; 2, F. De Paolis3; 4, A.A. Nucita3; 4, A.L. Kashin1, A. Amekhyan1, S. Sargsyan1, G. Yegorian1, A. Qadir5, G. Ingrosso3; 4, Ph. Jetzer6, and D. Vetrugno7 1 Center for Cosmology and Astrophysics, Alikhanian National Laboratory and Yerevan State University, Yerevan, Armenia 2 SIA, Sapienza University of Rome, Rome, Italy 3 Dipartimento di Matematica e Fisica “E. De Giorgi”, Università del Salento, Via per Arnesano, I-73100, Lecce, Italy 4 INFN, Sezione di Lecce, Via per Arnesano, I-73100, Lecce, Italy 5 Department of Physics, School of Natural Sciences, National University of Sciences and Technology, Islamabad, Pakistan 6 Physik-Institut, Universität Zürich, Winterthurerstrasse 190, 8057 Zürich, Switzerland 7 Department of Physics, University of Trento, I-38123 Povo, Trento, Italy and TIFPA/INFN, I-38123 Povo, Italy Submitted: XXX; Accepted: XXX ABSTRACT This paper is a follow-up of a previous paper about the M82 galaxy and its halo based on Planck observations. As in the case of M82, so also for the M81 galaxy a substantial North-South and East-West temperature asymmetry is found, extending up to galactocentric distances of about 1:50. The temperature asymmetry is almost frequency independent and can be interpreted as a Doppler-induced effect related to the M81 halo rotation and/or triggered by the gravitational interaction of the galaxies within the M81 Group. Along with the analogous study of several nearby edge-on spiral galaxies, the CMB temperature asymmetry method thus is shown to act as a direct tool to map the galactic haloes and/or the intergalactic bridges, invisible in other bands or by other methods. Key words. Galaxies: general – Galaxies: individual (M81) – Galaxies: halos 1. Introduction the detected temperature asymmetries are always almost frequency independent is a strong indication of an effect Cosmic Microwave Background (CMB) data are mainly due to the galaxy rotation and remark the importance of used with the primary aim to infer the values of the parame- the methodology proposed which, in spite of its simplicity, ters of the cosmological standard model. In addition, CMB may allow one to consistently estimate the galaxy dynami- data also offer a unique opportunity to study the large-scale cal mass contained within a certain galactocentric distance. temperature asymmetries far beyond the size typically ac- We have also shown that, in general, our method, can be cessible with other tools toward nearby astronomical sys- applied to nearby nearly edge-on spirals and may be used tems (see, e.g., Rauzy & Gurzadyan 1998; De Paolis et al. to trace the halo bulk dynamics on rather large scales in a 2011). Here we continue the use of CMB data to map the model-independent way. The present paper is a follow-up dark haloes of nearby galaxies, the latter often studied in of the previous paper on the M82 galaxy (Gurzadyan et most details on other bands or via other methods. Indeed, al. 2015) where a substantial North-South and East-West in the recent past we have analyzed Planck data toward temperature asymmetry was found, extending up to about four nearby galaxies with the main aim of testing if mi- 10 from the M82 center. The main conclusion about the crowave data show a substantial temperature asymmetry origin of the temperature asymmetry (almost frequency- of one side with respect to the other about the rotation independent) was its link with a Doppler-induced effect re- axis of the galactic disks. We have considered, in partic- garding the line-of-sight dynamics on the real halo scale - ular: M31 galaxy and its halo (De Paolis et al. 2014) the invisible in other bands - the ejections from the galactic active radio galaxy Centaurus A (Cen A) that is considered arXiv:1710.04166v1 [astro-ph.GA] 11 Oct 2017 center or the tidal interaction of M82 with the M81 galaxy. the closest AGN (De Paolis et al. 2015), M82, the largest Here, we consider again this issue from the point of view of galaxy in the M81 Group in the Ursa Major constellation the M81 galaxy, one of the last objects in the Local Group (Gurzadyan et al. 2015), the M 33 galaxy where we found a which can be studied by available Planck data. substantial temperature asymmetry with respect to its mi- nor axis projected onto the sky plane which extends up to 0 about 3 from the galactic center and correlates well with 2. Planck data analysis and results toward M81 the HI velocity field at 21 cm, at least within about 0:50 (De Paolis et al. 2016). We emphasize that the very fact that M81, also known as Bode’s galaxy (or NGC 3031), at J2000 coordinates R.A.: 09h 55m 33.1730s, Dec: +690 Send offprint requests to: F. De Paolis, e-mail: 30 55.06100 (Galactic Longitude l = 142:09184060, Galac- [email protected] tic Latitude b = 40:90014090) is a SA(s)ab type galaxy at Article number, page 1 of 5 a distance of 3:6 ± 0:2 Mpc from us (see, e.g., Gerke et al. 2011). Following the procedures described in the pre- vious papers, we have used the publicly released Planck 2015 data1 Planck Collaboration I (2016) in the bands at 70 GHz of the Low Frequency Instrument (LFI), and in the bands at 100 GHz, 143 GHz and 217 GHz of the High Frequency Instrument (HFI). We have also used the foreground-corrected SMICA band (indicated as SmicaH in Figs. 2 and 3) which should display the lowest contam- ination by the galactic foregrounds. We notice here that Planck’s resolution is 13:20, 9:60, 7:10 and 50 in terms of FHWM at 70, 100, 143 and 217 GHz bands, respectively, and frequency maps (Planck Collaboration XVI 2016) are provided in CMB temperature at resolution corresponding to Nside=2048 in HEALPix scheme (Górski et al. 2005). To study in the simplest way the CMB data toward the Fig. 2. Upper panel: the temperature asymmetry toward M81 in µK (with the standard errors) of the A1+A2 region (indicated as A12) with respect to the A3+A4 region (A34) in the five considered Planck bands (see text for details) within three radial Fig. 1. The Planck field toward the M81 galaxy in the distances of 300 (R0:50), 600 (R1:00) and 900 (R1:50). Bottom 143 GHz band. The pixel color gives the temperature excess in panel: the same for the 360 control fields with the same geometry µK with respect to the mean CMB temperature. The optical (shown in Fig. 1) equally spaced at one degree distance to each extension of the M81 galaxy is indicated by the inner ellipse other in Galactic longitude and at the same latitude as M81. with apparent dimensions of 26:90 and 14:10, respectively. The four quadrants A1, A2, A3 and A4 are used in the analysis. 0 The thin dashed black line marks the Galactic latitude b = 40 0 North. We note that the M82 galaxy is clearly visible as the red about 50 − 70 µK within 1:5 . Note that the control fields spot in the A1 region at about 380 from the center of M81. show a much smaller temperature asymmetry of only a few µK and that the detected effect is practically the same in M81 galaxy, the Planck field of the region of interest (we any of the five Planck’s bands. We also note that the size of give in Fig. 1 the map in the case of the 143 GHz band) the virial radius of the M81 galaxy (equivalent to the R200 has been divided into four quadrants A1, A2, A3 and A4. radius where the galaxy density is about 200 times larger 0 As detailed in the histograms in Figs. 2 and 3 we have con- than the critical density) can be estimated to be about 3:6 sidered the temperature asymmetry in three radial regions (Chiboucas et al. 2009). Although from the geometry and about the M81 center within 0:50, 10 and 1:50 (indicated the direction rotation of the M81 disk, the expected tem- as R0.50, R1.00 and R1.50, respectively). In Fig. 1 the op- perature asymmetry was along the A12/A34 axis, we have tical extension of the M81 galaxy is shown, as indicated by also considered the temperature asymmetry toward M81 in the inner ellipse. In Fig. 2 we give the temperature asym- the A14 region with respect to the A23 region and found metry toward M81 in µK (with the standard errors) of the an even more consistent asymmetry in all the considered A1+A2 region (A12) with respect to the A3+A4 region Planck bands. This resembles what was already found to- (A34) in the five considered Planck bands within the three wards the companion galaxy M82 (Gurzadyan et al. 2015). radial distances. In the bottom panel we give the same for In the present case the temperature asymmetry amounts the 360 control fields with the same geometry (shown in to 40 − 80 µK as implied by a prolate M81 halo rotation, Fig. 1) equally spaced at one degree distance to each other while the control fields always show an asymmetry consis- in Galactic longitude and at the same latitude as M81. As tent to zero (see Fig. 3). As far as the foreground-corrected one can see from Fig. 2 and as expected by considering the SMICA band is concerned, the temperature asymmetry is 0 rotation direction of the M81 disk about its rotation axis, negligible within 0:5 (although one has to consider that The A12 region always appears hotter than the A34 region the pixel number in this region is very low) and increases 0 0 by 32 − 44 µK within 0:50, by 28 − 40 µK within 10 and by to large values within 1 and 1:5 .
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